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The SPIRou Legacy Survey: near-infrared and optical radial velocity analysis of Gl 480 and Gl 382 using SPIRou, HARPS and CARMENES spectrographs

T0 review · 3 major / 6 minor · reviewed 2026-08-08 · deepseek-v4-flash

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Pith's one-line read This paper confirms the 9.55-day super-Earth around Gl 480 by combining near-infrared and optical radial velocities, and finds that a tentative 6.4-day signal depends on how stellar activity is modeled.

desk verdict Solid survey paper that confirms a known 9.55 d planet with an improved—but possibly prior-dependent—mass, adds a fragile 6.4 d candidate, and gives a clean null result for Gl 382; the main soft spot is the untested common-K assumption across nIR/optical data. read the letter →

arxiv 2502.07086 v2 pith:KNQ3SRCU submitted 2025-02-10 astro-ph.EP astro-ph.SR

M. Ould-Elhkim , C. Moutou , J-F. Donati , É. Artigau , C. Cadieux , E. Martioli , T. Forveille , J. Gomes da Silva
show 8 more authors
R. Cloutier A. Carmona P. Fouqué P. Charpentier P. Larue N.J. Cook X. Delfosse R. Doyon
This is my paper · ORCID
classification astro-ph.EPastro-ph.SR
keywords radialvelocitiesMdwarfplanetsSPIRounear-infraredspectroscopyGaussianprocessregressionstellaractivityGl480382
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper tests whether two nearby M dwarfs host planets by combining near-infrared radial velocities from the SPIRou spectrograph with published optical velocities from HARPS and CARMENES. It confirms that Gl 480 hosts a super-Earth on a 9.5537-day orbit and revises its minimum mass down to 8.8 Earth masses, a value meaningfully different from the earlier 13.2 Earth masses. The same analysis uncovers a tentative 6.4-day signal that only crosses the detection threshold when stellar activity is modeled with priors taken from one activity indicator, so the paper treats it as unconfirmed. For Gl 382, no planet survives activity correction, and the dataset sets an upper mass limit of about 5.9 Earth masses for any companion in the habitable zone.

What carries the argument

The argument is carried by three components working in series: the line-by-line (LBL) extraction that turns SPIRou spectra into per-line radial velocities; the Wapiti method, a weighted principal-component analysis applied to those per-line time series to identify and subtract instrumental systematics; and quasi-periodic Gaussian-process regression on the radial-velocity time series to absorb stellar activity. The Gaussian process is the load-bearing piece for the weak signals, because its rotation period and smoothing hyperparameters are set from stellar activity indicators, and changing those priors changes whether the 6.4-day signal is detected.

What would settle it

A stacked periodogram of new high-cadence radial velocities of Gl 480 at 6.4 days would settle the candidate: if the signal is a planet, its log Bayes factor should rise steadily above 5 as observations accumulate, while an activity artifact would fluctuate or fade when the Gaussian-process priors are changed.

Watch

Extended reading notes

Core claim

The paper's central claim is that a joint analysis of SPIRou near-infrared and HARPS/CARMENES optical radial velocities, cleaned of instrumental systematics by the Wapiti weighted-principal-component correction and of stellar activity by quasi-periodic Gaussian processes, confirms one planet around Gl 480: period $9.5537 \pm 0.0005$ d, semi-amplitude $K = 4.5 \pm 0.3$ m s$^{-1}$, and minimum mass $8.8 \pm 0.7$ M$_\oplus$. It also reports that the previously claimed mass of $13.2 \pm 1.7$ M$_\oplus$ is not reproduced, and that a low-amplitude signal at $6.4$ d is present but not robust: its log Bayes factor rises above 5 only when the Gaussian-process priors come from the dLW activity indicator, and the signal is compatible with nondetection in the optical data. For Gl 382, the authors find that all radial-velocity variation is explained by stellar activity, and injection-recovery tests set an upper limit of $5.9 \pm 0.8$ M$_\oplus$ on a habitable-zone companion.

Load-bearing premise

The load-bearing premise is that the quasi-periodic Gaussian-process model with priors taken from the dLW activity indicator correctly separates stellar activity from the 6.4-day signal; if those priors misrepresent the star, that candidate disappears, though the 9.55-day planet would remain.

Editorial extensions

If this is right

  • If the 9.5537-day planet is real, Gl 480 b has a minimum mass near 8.8 Earth masses, placing it in the super-Earth regime with a likely equilibrium temperature around 406 K.
  • The revised mass is about 30 percent lower than the earlier HARPS/HIRES estimate, which would change any conclusions about the planet's bulk composition drawn from the older value.
  • If the tentative 6.4-day signal is confirmed by more data, the two periods lie close to a 3:2 commensurability, making the system interesting for orbital dynamics.
  • For Gl 382, the absence of signals above the injection-recovery threshold implies that any habitable-zone companion has minimum mass below about 5.9 Earth masses.
  • The paper's demonstration that activity priors decide the 6.4-day detection means future low-amplitude claims should report sensitivity to activity modeling choices.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Editorial inference: the prior-dependence of the 6.4-day signal suggests that many ultra-low-amplitude M-dwarf radial-velocity candidates may be similarly fragile, and reporting the full prior-sensitivity range is the right default for such claims.
  • Editorial inference: if the 6.4-day signal is real, the near 3:2 resonance with the 9.55-day planet would make Gl 480 a natural target for transit-timing searches if a transiting geometry is ever found.
  • Editorial inference: the 50-day signal seen in Gl 382's near-infrared and HARPS activity indicators but not in optical radial-velocity residuals hints that wavelength-dependent surface features affect radial velocities differently; a testable extension would be to model simultaneous optical and near-infrared epochs with the multi-dimensional Gaussian-process approach the paper names as future work
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 6 minor

Summary. This paper presents a radial-velocity (RV) analysis of two nearby M dwarfs, Gl 480 and Gl 382, combining near-infrared SPIRou data with optical HARPS and CARMENES data. The authors use the LBL framework, the Wapiti systematics-correction method, Bayesian periodograms, and quasi-periodic Gaussian-process models with several choices of priors. For Gl 480, they confirm the previously reported 9.5537 d planet and derive a joint-fit minimum mass of 8.8 +/- 0.7 Earth masses, significantly lower than the Feng et al. (2020) value of 13.2 +/- 1.7 Earth masses. They also report a tentative 6.4 d signal whose significance depends strongly on the GP prior choice. For Gl 382, no planetary signals are found, and they place an upper limit of about 5.9 Earth masses for companions in the habitable zone.

Significance. If the main result holds, the paper provides a useful multi-wavelength confirmation and an improved mass measurement for a known super-Earth around an M dwarf, and it demonstrates a careful systematics-correction pipeline for SPIRou data. The explicit injection-recovery test for the optical non-detection of the 6.4 d signal and the transparent reporting of prior sensitivity are commendable. The Gl 382 non-detection and detection-limit analysis are also valuable for the SLS planet-search program. However, the central mass claim rests on a common-semi-amplitude assumption that is not tested, and the tentative 6.4 d candidate is only significant under one set of activity-informed priors. These issues do not undermine the existence of the 9.5 d signal, but they do affect the headline mass and the status of the second signal.

major comments (3)
  1. [§3.1.4, Table 3] The headline mass M sin i = 8.8 +/- 0.7 Earth masses rests on the joint fit with a common semi-amplitude K_b = 4.5 +/- 0.3 m/s, while the SPIRou-only and optical-only fits give K_b = 3.6 +/- 0.5 and 5.0 +/- 0.5 m/s, a difference of about 2 sigma given the quoted uncertainties. The statement in §3.1.3 that the difference is 'within 5 sigma' is not a quantitative compatibility test, and the paper never fits a model with separate K_b for the nIR and optical data. Because the claimed improvement over Feng et al. (2020) depends on this joint value, the authors should either report a separate-K fit with its BIC and parameters, or otherwise demonstrate that the common-K assumption does not bias the period and mass.
  2. [§3.1.2, §3.1.4, Table 3] The 6.4 d signal is only significant when the SPIRou GP uses Priors III, whose hyperparameters are derived from the dLW activity time series of the same star. In the SPIRou-only analysis the log BF is 2.31, 1.90, and 3.71 for Priors I, II, and III, all below the adopted threshold of 5; in the combined fit the signal reaches log BF = 6.7 only with Priors III, while remaining below threshold with Priors I and II. Because the prior set was chosen partly on the basis of BIC for the same dataset that contains the candidate, the reported significance is not robust. The manuscript should present the 6.4 d significance and parameters for all prior sets in the main text and should clearly label Gl 480 c as a prior-dependent candidate rather than listing it as a planet in the final parameter table.
  3. [§2.4] The removal of four outliers from the Gl 480 SPIRou dataset is described without any objective rejection criterion. Since the 9.5 d semi-amplitude is only about 3.6 m/s, a handful of points can influence the fitted K and thus the derived planet mass. Please state the outlier criterion (for example, a residual threshold, a bad-pixel flag, or an instrumental issue) and show that the main results are unchanged when the outliers are retained.
minor comments (6)
  1. [Table 5] The table caption says 'Gl 480' but the table contains parameters for Gl 382; the caption should be corrected.
  2. [Section 4] The conclusion contains a duplicated phrase: 'to better constrain its orbital parameters., this signal could not be detected with these data.' The second clause appears to be a copy-paste error and should be removed.
  3. [§2.2, §3.2.1, Figure 8, Acknowledgements] There are several typographical errors: 'Eath' should be 'Earth', 'rotatinoal' should be 'rotational', 'twp panels' should be 'two panels', and 'acknoweldge' should be 'acknowledge'.
  4. [§3.1.3] The phrase 'within 5 sigma' for the nIR/optical semi-amplitude difference is misleading; with the quoted errors the difference is approximately 2 sigma. Please quantify the compatibility properly or reword.
  5. [Figure 5 caption] The caption refers to 'planets 1 and 2', but the 6.4 d signal is described elsewhere as tentative; using 'signals' or 'candidate' would be more consistent with the paper's own caveats.
  6. [§3.1.4] The statement that the individual datasets 'do not overlap' is ambiguous; the authors likely mean that the time baselines of the optical datasets do not overlap with the long SPIRou baseline or that the observations are not simultaneous. Please clarify.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the 9.5 d planet signal is recovered in two independent instrument families and compared with a prior independent detection, while the prior-dependent 6.4 d candidate is transparently flagged as tentative.

full rationale

The derivation chain is self-contained and does not reduce any claimed result to its own inputs by construction. The 9.5 d signal is detected independently in the SPIRou nIR time series and in the HARPS+CARMENES optical time series (Sections 3.1.2-3.1.4), and it reproduces the earlier independent detection of Feng et al. (2020); the quoted period and mass therefore rest on cross-instrument data, not on a fitted parameter renamed as a prediction. The paper explicitly acknowledges the ~2 sigma discrepancy between the SPIRou-only K = 3.6 +/- 0.5 m/s and optical K = 5.0 +/- 0.5 m/s entries of Table 3, writing that 'this discrepancy is not caused by either the Wapiti correction or the GP applied on SPIRou data' and that it 'could raise some uncertainty about the true planetary nature of this signal'; a common-K joint fit is a stated modeling choice, not a hidden construction. The tentative 6.4 d signal is likewise presented with its sensitivity exposed: 'the statistical significance of this signal depends critically on the choice of prior distributions in our quasi-periodic GP models,' and the paper reports log BF values below threshold for Priors I and II (Section 3.1.4), so the detection is explicitly prior-dependent rather than claimed as robust. The Wapiti and GP machinery cites the authors' prior methodology (Ould-Elhkim et al. 2023; Artigau et al. 2022, 2024), but those are tool and method papers whose operation is described in this manuscript, and the central planet claim does not rest on an unverified uniqueness theorem or on an ansatz smuggled in by citation. Stellar parameters from Cristofari et al. (2022) enter the mass conversion, but they are externally anchored stellar characterizations, not the target detection. Hence no step satisfies the circularity criteria; score 0.

Assumptions & free parameters 3 free parameters · 4 assumptions · 1 invented entities

The central load-bearing choices are the Wapiti component selection and the GP prior sets. The 9.5 d planet itself does not depend on these choices, but the 6.4 d candidate does. The ledger reflects that the paper's new detections are conditioned on model assumptions rather than on new physical entities.

free parameters (3)
  • GP hyperparameters (amplitude A, decay λ, smoothing Γ, rotation period P_rot) = e.g., P_rot=49.7 to 52 d (Gl 480), 20.8 d (Gl 382)
    Fitted via MCMC; the 6.4 d candidate's significance changes with prior choice, so these parameters control the central result.
  • Number of Wapiti components = 1 for Gl 480; 4 for Gl 382 (selected order V6,V2,V5,V7)
    Selected by BIC; changing the component count alters the residuals and could hide or create signals.
  • Removed outliers (Gl 480) = 4 points
    Removed before Wapiti correction without a stated statistical criterion; affects the 9.5 d amplitude estimate.
assumptions (4)
  • domain assumption LBL RVs from APERO-reduced SPIRou spectra are accurate after drift and nightly zero-point correction
    Section 2.1 relies on pipeline calibration, telluric correction, and reference stars without showing calibration validation for these targets.
  • domain assumption Wapiti wPCA components represent instrument systematics and do not absorb planetary signals
    Section 2.4 applies wPCA to the same RV time series used for planet searches; no injection test is performed to verify that a planetary signal survives the correction.
  • domain assumption Quasi-periodic GP kernel with priors from activity indicators adequately models stellar activity
    Sections 3.1.2 and 3.2.2 use GP priors from dET/dLW; the 6.4 d detection is only significant for one prior set, so the kernel/prior choice is load-bearing.
  • ad hoc to paper log BF > 5 is a valid detection threshold
    Adopted from Delisle et al. 2018; the 6.4 d signal sits near this threshold and the threshold itself is conventional, not derived.
invented entities (1)
  • Gl 480 c, a 6.4 d planet candidate with M sin i ≈ 2.7 M⊕
    purpose: Explains a residual RV signal in the combined nIR+optical dataset
    The signal's significance depends on the GP prior choice (only Priors III gives log BF=6.7) and it is not recovered by optical data alone (19% recovery in injection-recovery simulations).

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Cite this review

Pith. "Pith review of The SPIRou Legacy Survey: near-infrared and optical radial velocity analysis of Gl 480 and Gl 382 using SPIRou, HARPS and CARMENES spectrographs." pith.science (2026). https://pith.science/paper/KNQ3SRCU

@misc{pith2026250207086,
  author       = {Pith},
  title        = {Pith review of: The SPIRou Legacy Survey: near-infrared and optical radial velocity analysis of Gl 480 and Gl 382 using SPIRou, HARPS and CARMENES spectrographs},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/KNQ3SRCU}},
  note         = {Machine review of arXiv:2502.07086}
}
abstract

Context: Advancements in the field of exoplanetary research have extended radial velocity (RV) observations from the optical to the near-infrared (nIR) domain. M dwarf stars, characterized by their lower masses and higher prevalence of rocky planets, have become a focal point of investigation. This study uses data from the near-infrared spectropolarimeter SPIRou and data available in the literature from the HARPS and CARMENES spectrographs operating in the optical to analyze RVs of two nearby M dwarfs, Gl 480 and Gl 382. Aims: This work aims to detect and characterize exoplanetary companions around Gl 480 and Gl 382 by mitigating stellar activity effects through advanced data analysis techniques. The study seeks to improve the reliability of RV signals by integrating multi-wavelength observations and stellar activity diagnostics. Methods: The study employs a comprehensive approach that combines the line-by-line (LBL) framework with the Wapiti (Weighted principAl comPonent analysIs reconsTructIon) method to correct for systematics in SPIRou data. Through an extensive analysis of available stellar activity indicators and by combining optical data from the HARPS and CARMENES instruments, we perform a joint analysis of RV measurements in both the nIR and optical domains. Results: Our analysis confirms the detection of a planet orbiting Gl 480 with a period of $9.5537 \pm 0.0005$ d and a minimum mass of $8.8 \pm 0.7$ M$_\oplus$. Additionally, we detect a tentative signal at 6.4 d, whose significance depends strongly on the choice of Gaussian Process priors constrained by stellar activity indicators and would require further observations for confirmation. In contrast, no planetary signals are detected for Gl 382, where RV variations are dominated by stellar activity.

Figures

Figures reproduced from arXiv: 2502.07086 by the authors.

Figure 1
Figure 1. Bayesian periodograms of various stellar activity indicators of Gl 480. In order dLW, Hα and the NaD1 index time series from HARPS data, and the dLW, Bℓ and dET time series from SPIRou data. The dashed green lines in the bottom panel mark periodicities at the stellar rotation period (Prot), half rotation period (Prot/2), and one-third rotation period (Prot/3). The significance level of log BF “ 5 is indicated by the… view at source ↗
Figure 2
Figure 2. Iterative search of signals with Bayesian periodograms using SPIRou data of Gl 480. The top four panels display log BF periodograms for (a) raw data, (b) Wapiti correction, (c) Planet b model fit, and (d) long term and/or stellar activity correction. The dashed green lines in the bottom panel mark periodicities at the stellar rotation period (Prot), half rotation period (Prot/2), and one-third rotation period (Prot/… view at source ↗
Figure 3
Figure 3. Iterative search of signals with Bayesian periodograms using HARPS and CARMENES data of Gl 480. The three panels display log BF periodograms for (a) raw data, (b) Planet b model fit, and (c) stellar activity correction. The dashed green lines in the bottom panel mark periodicities at the stellar rotation period (Prot), half rotation period (Prot/2), and one-third rotation period (Prot/3). The significance level of l… view at source ↗
Figures from the paper (7 more)
Figure 4
Figure 4. Figure 4: Histogram of the maximum log BF values of the injected period in the injection-recovery simulations. The solid red line indicates the log BF value of 1.8 retrieved from the residuals of the real datasets, while the dashed red line marks the detection threshold at log B…
Figure 5
Figure 5. Figure 5: Final RV model for Gl 480. The top panel shows the raw RV data with offsets removed, plotted for SPIRou, HARPS, and CARMENES instruments (RMS = 5.92 m.s´1 ). The second and fourth rows display the contributions of planets 1 and 2 to the RV signal, respectively, along w…
Figure 6
Figure 6. Figure 6: Bayesian periodograms of various stellar activity indicators of Gl 382. In order the Ca II IRT 1, 2, 3, dLW, Hα and the NaD1 index time series from CARMENES data; the dLW, Hα and the NaD1 index time series from HARPS data; and the dLW, Bℓ and dET time series from SPIRo…
Figure 7
Figure 7. Figure 7: Iterative search of signals with Bayesian periodograms using SPIRou data of Gl 382. The top four panels display log BF periodograms for (a) raw data, (b) Wapiti correction, and (c) stellar activity correction. The dashed green lines in the bottom panel mark periodiciti…
Figure 8
Figure 8. Figure 8: Iterative search of signals with Bayesian periodograms using HARPS and CARMENES data of Gl 382. The twp panels display log BF periodograms for (a) raw data, (b) stellar activity correction. The dashed green lines in the bottom panel mark periodicities at the stellar ro…
Figure 9
Figure 9. Figure 9: Results of the injection-recovery test assessing the detectability of a planetary signal in the dataset. The top panel shows the detection rate as a function of orbital period and semi-amplitude, with colors representing the percentage of successful detections. The red…
Figure 10
Figure 10. Figure 10: Final RV model for Gl 382. The top panel shows the raw RV data with offsets removed, plotted for SPIRou, HARPS, and CARMENES instruments (RMS = 5.79 m.s´1 ). The second row illustrates the correction for stellar activity using GPs, with individual GP contributions sho…

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Pith tools

Reviewed August 8, 2026 · model on record in the stance chip above.